Discovery of PSR J0125-5854, a 24 ms pulsar in a binary with orbital period ~834 days, low eccentricity, and likely helium white dwarf companion.
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NE2025: An Updated Electron Density Model for the Galactic Interstellar Medium
13 Pith papers cite this work. Polarity classification is still indexing.
13
Pith papers citing it
abstract
Free electrons in the Galactic interstellar medium (ISM) disperse and scatter coherent radio waves, by amounts that depend on the distance to the radio source. Models of the Galactic electron density are thus widely used to predict distances and scattering of compact radio sources (including pulsars, fast radio bursts (FRBs), and long-period transients), in addition to mitigating ISM foregrounds in Galactic and extragalactic studies. We use a sample of 171 precise pulsar distances, based entirely on parallaxes and globular cluster associations, as well as scattering measurements of 568 pulsars, active galactic nuclei, and masers, to update the NE2001 Galactic electron density model. We refit the thick and thin disks and three of the spiral arms. The new parameters for these large-scale components significantly repartition free electrons between the thick disk and spiral arms, thereby correcting NE2001's systematic underestimation of pulsar distance and scattering. Sightlines with excessive dispersion and scattering are used to identify new clumps that are added to the model, in addition to refining clumps that were already included (e.g., Cygnus, Vela, and Gum). The Galactic Center component is revised, yielding scattering time predictions that are $10^3$ times smaller than the Galactic Center in NE2001. The updated model, NE2025, provides a factor of $20\times$ improvement in median distance prediction accuracy and $100\%$ median improvement in scattering predictions based on DM, relative to NE2001. There is a $15\times$ improvement in median distance prediction accuracy relative to YMW16. NE2025 is available on Github and the Python Package Interface.
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2026 13representative citing papers
First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
RRATs number up to 400000 in the Galaxy with a birth rate of at most 1.4 per century, comparable in size to pulsars at high luminosities and consistent with supernova rates.
FRB dispersion measures reveal a large-scale excess of ionized gas in the northern sky spatially aligned with the Ursa Major supercluster.
A polarization catalog of 6,131 bursts from FRB 20240114A reveals linearly decreasing rotation measure, stable dispersion measure, high linear polarization fractions, low circular polarization, and a broad distribution of intrinsic polarization angles, indicating a dynamically evolving magneto-ionic
A phase-coherent 20-year timing solution for PSR J1905+0154A yields precise spin, orbital and astrometric parameters, identifies a helium white dwarf companion of 0.17-0.19 solar masses, and indicates the system may be unbound from NGC 6749.
Simulations indicate HI absorption in FRB spectra is detectable when scintillation decorrelation bandwidth differs markedly from absorption width, with ≳1000 stacked bursts needed at current sensitivities.
A 9-hour FAST observation covering ~4230 GCs in M49 found no FRBs and sets an upper limit of 4.7e-4 FRB GC^-1 hr^-1 above ~16.5 mJy ms fluence.
Analysis of CHIME/FRB Catalog 2 with synthetic injections and a multidimensional selection function yields evidence for a slight downturn in the intrinsic scattering timescale distribution, though flat or rising distributions remain possible.
Forecasts using mock CSST lensing and SKA/DSA-2000 FRB DM data show joint analysis improves log10 T_AGN precision from 3.1% to 0.4% and tightens sum m_nu upper limit to <0.47 eV.
Updated timing of PSR J1913+1102 yields threefold better total mass precision and fivefold better intrinsic orbital decay, consistent with general relativity and constraining dipolar gravitational wave emission plus scalarisation near 1.6 solar masses.
PATH is extended with three fitted P(m_r|z) prior models combined with P(z|DM), raising host-association confidence for ASKAP FRBs while showing fainter-than-expected host magnitude distribution.
The paper describes the expected capabilities of the SKA-Mid survey to produce a complete map of the Milky Way's magnetic field in the southern hemisphere using rotation measures and polarized emission.
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The magnetic field in the Milky Way Galaxy: from large to small scales
The paper describes the expected capabilities of the SKA-Mid survey to produce a complete map of the Milky Way's magnetic field in the southern hemisphere using rotation measures and polarized emission.